Uv Imaging of Optical Jets: a New Window on the Physics of Jets

Details Uv Imaging of Optical Jets: a New Window on the Physics of Jets Uv Imaging of Optical Jets: a New Window on the Physics of Jets

Jul 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999hst..prop.8233b&link_type=abstract

HST Proposal ID #8233

Physics

Hst Proposal Id #8233 Agn Physics

Scientific paper

Extragalactic radio jets are highly collimated beams of high energy particles and magnetic fields issuing forth at relativistic speeds from sub-parsec scale regions, extending hundreds of kpc through interstellar and intergalactic space. They are unique in their scope, power, and size. The jets affect their host galaxies and environments, through kinetic energy output and through deposition of cosmic rays and magnetic fields into interstellar and intergalactic space. Despite years of study, fundamental jet parameters such as the magnetic field strength, particle density, jet configuration, bulk Lorentz factor, and the nature of particle acceleration in the flow remain unknown. Determining these key parameters and how they vary in different sources is key to formulating a theory of the physics of the creation and propagation of these jets. The tightest constraints on the physics of jets come not from radio observations, but from observations in the optical, UV, and x-ray, where the lifetimes of the synchrotron emitting particles are measured in hundreds of years and the particles travel distances of hundreds of parsecs. We propose to use the unique advantage of STIS' UV sensitivity and high spatial resolution to obtain images at 1400Angstrom and 2400Angstrom of a sample of seven optically-emitting radio jets. This dataset will provide qualitatively new data with which to constrain the physics of extra-galactic jets.

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